Abstract
Outflows are a pervasive feature of mechanical feedback from super star clusters (SSCs) in starburst galaxies, playing a fundamental role in galaxy evolution. Observations are now starting to confirm that outflows can undergo catastrophic cooling, suppressing adiabatic superwinds. Here we present a suite of one-dimensional, hydrodynamic simulations that study the ionization structure of these outflows and the resulting line emission generated by the cooling gas. We use the non-equilibrium atomic chemistry package within MAIHEM, our modified version of FLASH, which evolves the ionization state of the gas and computes the total cooling rate on an ion-by-ion basis. We find that catastrophically cooling models produce strong nebular line emission compared to adiabatic outflows. We also show that such models exhibit non-equilibrium conditions, thereby generating more highly ionized states than equivalent equilibrium models. When including photoionization from the parent SSC, catastrophically cooling models show strong C iv λ1549 and O vi λ1037 emission. For density-bounded photoionization, He ii λ1640, λ4686, C iii] λ1908, Si iv λ1206, and Si iii λ1400 are also strongly enhanced. These lines are seen in extreme starbursts where catastrophic cooling is likely to occur, suggesting that they may serve as diagnostics of such conditions. The higher ionization generated by these flows may help to explain line emission that cannot be attributed to SSC photoionization alone.
Original language | English (US) |
---|---|
Article number | 161 |
Journal | Astrophysical Journal |
Volume | 887 |
Issue number | 2 |
DOIs | |
State | Published - Dec 20 2019 |
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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Catastrophic Cooling in Superwinds : Line Emission and Non-equilibrium Ionization. / Gray, William J.; Oey, M. S.; Silich, Sergiy et al.
In: Astrophysical Journal, Vol. 887, No. 2, 161, 20.12.2019.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Catastrophic Cooling in Superwinds
T2 - Line Emission and Non-equilibrium Ionization
AU - Gray, William J.
AU - Oey, M. S.
AU - Silich, Sergiy
AU - Scannapieco, Evan
N1 - Funding Information: William J. Gray M. S. Oey Sergiy Silich Evan Scannapieco William J. Gray M. S. Oey Sergiy Silich Evan Scannapieco Department of Astronomy, University of Michigan, 1085 South University Ave., Ann Arbor, MI 48109, USA CLASP, College of Engineering, University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109, USA Instituto Nacional de Astrof�sica, Optica, y Electr�nica, Puebla, AP 51, 72000 Puebla, Mexico School of Earth and Space Exploration, Arizona State University, USA William J. Gray, M. S. Oey, Sergiy Silich and Evan Scannapieco 2019-12-20 2019-12-17 16:23:30 cgi/release: Article released bin/incoming: New from .zip NASA HST-GO- 14080.002-A CONACYT-Mexico A1-S-28458 National Science Foundation AST-1715876 yes Outflows are a pervasive feature of mechanical feedback from super star clusters (SSCs) in starburst galaxies, playing a fundamental role in galaxy evolution. Observations are now starting to confirm that outflows can undergo catastrophic cooling, suppressing adiabatic superwinds. Here we present a suite of one-dimensional, hydrodynamic simulations that study the ionization structure of these outflows and the resulting line emission generated by the cooling gas. We use the non-equilibrium atomic chemistry package within MAIHEM , our modified version of FLASH , which evolves the ionization state of the gas and computes the total cooling rate on an ion-by-ion basis. We find that catastrophically cooling models produce strong nebular line emission compared to adiabatic outflows. We also show that such models exhibit non-equilibrium conditions, thereby generating more highly ionized states than equivalent equilibrium models. When including photoionization from the parent SSC, catastrophically cooling models show strong C iv λ 1549 and O vi λ 1037 emission. For density-bounded photoionization, He ii λ 1640, λ 4686, C iii ] λ 1908, Si iv λ 1206, and Si iii λ 1400 are also strongly enhanced. These lines are seen in extreme starbursts where catastrophic cooling is likely to occur, suggesting that they may serve as diagnostics of such conditions. The higher ionization generated by these flows may help to explain line emission that cannot be attributed to SSC photoionization alone. � 2019. The American Astronomical Society. All rights reserved. Agertz O. and Kravtsov A. V. 2015 ApJ 804 18 10.1088/0004-637X/804/1/18 Agertz O. and Kravtsov A. V. ApJ 0004-637X 804 1 18 2015 18 Amorín R., Fontana A., Pérez-Montero E. et al 2017 NatAs 1 0052 10.1038/s41550-017-0052 Amorín R., Fontana A., Pérez-Montero E. et al NatAs 1 2017 0052 Amorín R., Pérez-Montero E., Vílchez J. M. and Papaderos P. 2012 ApJ 749 185 10.1088/0004-637X/749/2/185 Amorín R., Pérez-Montero E., Vílchez J. M. and Papaderos P. ApJ 0004-637X 749 2 185 2012 185 Badnell N. 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PY - 2019/12/20
Y1 - 2019/12/20
N2 - Outflows are a pervasive feature of mechanical feedback from super star clusters (SSCs) in starburst galaxies, playing a fundamental role in galaxy evolution. Observations are now starting to confirm that outflows can undergo catastrophic cooling, suppressing adiabatic superwinds. Here we present a suite of one-dimensional, hydrodynamic simulations that study the ionization structure of these outflows and the resulting line emission generated by the cooling gas. We use the non-equilibrium atomic chemistry package within MAIHEM, our modified version of FLASH, which evolves the ionization state of the gas and computes the total cooling rate on an ion-by-ion basis. We find that catastrophically cooling models produce strong nebular line emission compared to adiabatic outflows. We also show that such models exhibit non-equilibrium conditions, thereby generating more highly ionized states than equivalent equilibrium models. When including photoionization from the parent SSC, catastrophically cooling models show strong C iv λ1549 and O vi λ1037 emission. For density-bounded photoionization, He ii λ1640, λ4686, C iii] λ1908, Si iv λ1206, and Si iii λ1400 are also strongly enhanced. These lines are seen in extreme starbursts where catastrophic cooling is likely to occur, suggesting that they may serve as diagnostics of such conditions. The higher ionization generated by these flows may help to explain line emission that cannot be attributed to SSC photoionization alone.
AB - Outflows are a pervasive feature of mechanical feedback from super star clusters (SSCs) in starburst galaxies, playing a fundamental role in galaxy evolution. Observations are now starting to confirm that outflows can undergo catastrophic cooling, suppressing adiabatic superwinds. Here we present a suite of one-dimensional, hydrodynamic simulations that study the ionization structure of these outflows and the resulting line emission generated by the cooling gas. We use the non-equilibrium atomic chemistry package within MAIHEM, our modified version of FLASH, which evolves the ionization state of the gas and computes the total cooling rate on an ion-by-ion basis. We find that catastrophically cooling models produce strong nebular line emission compared to adiabatic outflows. We also show that such models exhibit non-equilibrium conditions, thereby generating more highly ionized states than equivalent equilibrium models. When including photoionization from the parent SSC, catastrophically cooling models show strong C iv λ1549 and O vi λ1037 emission. For density-bounded photoionization, He ii λ1640, λ4686, C iii] λ1908, Si iv λ1206, and Si iii λ1400 are also strongly enhanced. These lines are seen in extreme starbursts where catastrophic cooling is likely to occur, suggesting that they may serve as diagnostics of such conditions. The higher ionization generated by these flows may help to explain line emission that cannot be attributed to SSC photoionization alone.
UR - http://www.scopus.com/inward/record.url?scp=85077612056&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85077612056&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab510d
DO - 10.3847/1538-4357/ab510d
M3 - Article
AN - SCOPUS:85077612056
VL - 887
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 161
ER -